CCD Photometry of a Newly Confirmed SU UMa-Type Dwarf Nova, NSV 4838

Abstract

We present time-resolved CCD photometry of a dwarf nova NSV 4838 (UMa 8, SDSS J102320.27+440509.8) during the 2005 June and 2007 February outburst. Both light curves showed superhumps with a mean period of 0.0699(1) days for the 2005 outburst and 0.069824(83) days for the 2007 outburst, respectively. Using its known orbital period of 0.0678 days, we estimated the mass ratio of the system to be $q$=0.13 based on an empirical relation. Although the majority of SU UMa-type dwarf novae having similar superhump periods show negative period derivatives, we found that the superhump period increased at $\dot{P}$ / $P_{\mathrm{sh}}$=+7(+3, -4)$\times 10^{-5}$ during the 2007 superoutburst. We also investigated long-term light curves of NSV 4838, from which we derived 340 days as a supercycle of this system.

arXiv comment8 pages, 9 figures, accepted for PASJ

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Cited by in corpus (4)

• Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae
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• The Kepler light curves of V1504 Cygni and V344 Lyrae: A study of the Outburst Properties
• Spectroscopic Orbital Periods for 29 Cataclysmic Variables from the Sloan Digital Sky Survey